Radiation pressure
Radiation pressure is the pressure exerted upon any surface exposed to electromagnetic radiation. If absorbed, the pressure is the energy flux density divided by the speed of light.
Radiation Pressure
Electromagnetic radiation exerts a minute pressure on everything it encounters. This is known as radiation pressure, and can be thought of as the transfer of momentum from photons as they strike the surface of the object.
Radiation pressure is a physical pressure exerted by photons on matter. Even though photons are massless, they have an intrinsic momentum, hν/c, which is able to impart a force.
Radiation pressure
Wikipedia, the free encyclopedia - Cite This Source ...
RADIATION PRESSURE - Minute pressure exerted by electromagnetic radiation on everything it encounters. This can be thought of as the transfer of momentum from photons as they strike the surface of the object.
radiation pressure
a very small amount of pressure exerted on a surface by light or other electromagnetic radiation
radio galaxy ...
radiation pressure
The force exerted on an object by light particles (photons).
radiation zone
The inner region of the solar interior.
Radiation Pressure
The force exerted on the surface of a body by its absorption of light. Small particles floating in the solar system can be blown outward by the pressure of sunlight.
Radio Galaxy ...
see Radiation Pressure [H76]
Light-Time
The interval of time required for light to travel from a celestial body to the Earth.
radiation pressure The transfer of momentum carried by electromagnetic radiation to a body that the radiation impinges upon.
radio Region of the electromagnetic spectrum corresponding to radiation of the longest wavelengths. [More Info] ...
radiation pressure - (n.)
Pressure created by light hitting a surface.
radiative transport - (n.) ...
The Sun's radiation pressure and solar wind accelerate materials away from the comet's head at differing velocities according to the size and mass of the materials. Thus, relatively massive dust tails are accelerated slowly and tend to be curved.
Main article: Radiation pressure
Light pushes on objects in its path, just as the wind would do. This pressure is most easily explainable in particle theory: photons hit and transfer their momentum.
radiation pressure (NASA Thesaurus / NASA SP-7, 1965) (symbol Pr)
Pressure exerted upon any material body by electromagnetic radiation incident upon it. See Poynting-Robertson effect.
The new, increased radiation pressure actually causes the outer layers of the star to expand to maintain the pressure gradient. As the gas expands it cools, just as a spray can feels colder after use as the gas has been released.
acoustic radiation pressure (NASA SP-7, 1965) A unidirectional, steady-state pressure exerted upon a surface exposed to a sound wave.
The inward forces on each shell consist of the gravitational pull from all the shells inside it, and the gas and radiation pressure on the outside of the shell.
Interestingly, most dust grains in the disk are not agglomerating to form larger bodies; instead, they are eroding and being moved away from the star by radiation pressure when their size goes below about 2-10 microns.
dwarf, the class is deceptive, as Mu Ori Aa is a "metallic line" star, one whose spectrum is enhanced in various metals and depleted in others as a result of atmospheric diffusion, some chemical elements rising under the action of radiation pressure, ...
The dust is blown away from the coma by radiation pressure from the sunlight absorbed by individual dust grains.
The streams of dust and gas thus released form a huge, extremely tenuous atmosphere around the comet called the coma, and the force exerted on the coma by the Sun's radiation pressure and solar wind cause an enormous tail to form, ...
This is the luminosity at which, for uniform spherical accretion, the radiation pressure on accreting material balances the gravitational force and thus stops further accretion.
Stars with too much mass have so much radiation pressure inside pushing outward on the upper layers, that the star is unstable. It blows off the excess mass. The limit is about 100 solar masses.
The dust tail is comprised of dust particles pushed out of the coma by solar radiation pressure. The long white curving tail so often photographed from Earth is the dust tail.
Together with the radiation pressure generated by the photons, they exert pressure pushing outward to balance gravity's inward pull. Then, a star becomes stable and now enters the main sequence phase.
The H-R diagram and the Main Sequence Phase ...
Original estimates had the orbit lasting for 2000 years, but it was discovered that solar radiation pressure and atmospheric drag during high levels of solar activity produced significant perturbations in the perigee height of the satellite, ...
Radiation pressure, the pressure of sunlight, forces the dust particles back into a dust tail in the direction opposite to the Sun. A comet's tail can be tens of millions of kilometers in length when seen in the reflected sunlight.
Solar sails, which use solar radiation pressure in much the same way that a sailboat uses wind, promise to provide the means for high-speed interplanetary or interstellar propulsion. Here are some interesting solar-sailing links: ...
Space drive: Radiation pressure from intense radio waves has been proposed as a propulsion method for interstellar probes.
Scientists have been thinking about a variety of causes, such as the gravitational attraction of planets or even unknown dark matter; radiation pressure when photons hit the spacecraft; interaction between the solar wind and the spacecraft; ...
The ion tail also points away from the Sun because of the repulsive force exerted by solar radiation pressure on the minute particles. Larger particles released from the nucleus take up orbits that have nearly the same parameters as the parent comet.
Any gas remaining between the planets was blown away into interstellar space by the solar wind and the Sun's radiation pressure when the Sun entered this phase, just before nuclear burning started at its center.
"The filaments are made of dust and gravel, presumably recently thrown out of the nucleus. Some are swept back by radiation pressure from sunlight to create straight dust streaks.
If the comet gets close enough to the Sun, radiation pressure from sunlight pushes some of the dust away from the Sun, creating a long tail of dust.
It is straight and oriented radially away from the due to the solar wind. In type II comets, the dust tail (which is diffuse and steady) is generated by material subliming from the nucleus. The dust tail is pushed outwards by radiation pressure from ...
This is presumably caused by a build-up of carbon dust in the star's atmosphere, followed by the dust being dispersed by radiation pressure. The star is also known as the Fade-Out star or Reverse Nova.
 See also: Pressure, Light, Sun, Mass, Time
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